Temperature-dependent oscillation modes in rotating superfluid neutron stars

Abstract

We calculate the spectrum of inertial oscillation modes in a slowly rotating superfluid neutron star, including, for the first time, both the effects of finite temperatures and entrainment between superfluid neutrons and protons. We work in the Newtonian limit and assume minimal core composition (neutrons, protons and electrons). We also developed an approximate method that allows one to calculate the superfluid r-mode analytically. Finally, we derive and analyze dispersion relations for inertial modes in the superfluid NS matter in the short wavelength limit.

arXiv comment15 pages, 7 figures, accepted for publication in MNRAS

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Cited by in corpus (7)

• Bulk viscosity in neutron stars with hyperon cores
• Constraining neutron superfluidity with $r$-mode physics
• ${}^1$S${}_0$ pairing gaps, chemical potential and entrainment matrix in superfluid neutron-star cores for the Brussels-Montreal functionals
• Entrainment effects in neutron-proton mixtures within the nuclear-energy density functional theory. II. Finite temperatures and arbitrary currents
• Resonance suppression of the r-mode instability in superfluid neutron stars: Accounting for muons and entrainment
• Instability windows of relativistic r-modes in stably stratified neutron stars with hyperonic cores
• Extending Israel and Stewart hydrodynamics to relativistic superfluids via Carter's multifluid approach